3D simulations of pillars formation around HII regions: the importance of shock curvature

TL;DR

This paper uses 3D hydrodynamical simulations to show how shock curvature caused by interface modulations influences pillar formation at HII region edges, highlighting the importance of shock dynamics in structure development.

Contribution

It introduces a detailed model of ionization and shock interactions, emphasizing the role of shock curvature in pillar formation around HII regions.

Findings

Shock curvature is crucial for pillar formation.

Narrower initial interface modulations produce longer pillars.

Density modulations influence shock curvature and structure morphology.

Abstract

Radiative feedback from massive stars is a key process to understand how HII regions may enhance or inhibit star formation in pillars and globules at the interface with molecular clouds. We aim to contribute to model the interactions between ionization and gas clouds to better understand the processes at work. We study in detail the impact of modulations on the cloud-HII region interface and density modulations inside the cloud. We run three-dimensional hydrodynamical simulations based on Euler equations coupled with gravity using the HERACLES code. We implement a method to solve ionization/recombination equations and we take into account typical heating and cooling processes at work in the interstellar medium and due to ionization/recombination physics. UV radiation creates a dense shell compressed between an ionization front and a shock ahead. Interface modulations produce a curved shock that collapses on itself leading to stable growing pillar-like structures. The narrower the initial interface modulation, the longer the resulting pillar. We interpret pillars resulting from density modulations in terms of the ability of these density modula- tions to curve the shock ahead the ionization front. The shock curvature is a key process to understand the formation of structures at the edge of HII regions. Interface and density modulations at the edge of the cloud have a direct impact on the morphology of the dense shell during its formation. Deeper in the cloud, structures have less influence due to the high densities reached by the shell during its expansion.